The 1/4-keV diffuse soft X-ray background (SXRB) apparently
originates in a thermal plasma at around 106 K, but the
location of this emission has proven to be difficult to
determine. The finite flux in the Galactic plane and
similarity of the spectrum at all latitudes led to a model
where essentially all of the observed flux originated in a
local hot bubble (LHB) surrounding the Sun. Snowden et al.
(1998) have proposed a three-component model of the SXRB
from the ROSAT All-Sky Survey R12 (1/4 keV) map which
consists of an unabsorbed local component, an absorbed halo
component, and an absorbed power law to represent the known
contribution from AGN, which is quite small.

We have investigated whether this model is consistent with
the lower-energy data available from sounding rocket flights
in the B and Be bands. We find that the Snowden model
provides better correspondence with the low-energy Wisconsin
bands than the pure LHB model. The differences are subtle
because the bulk of the intensity variation in the Snowden
model is still due to differences in the extent of the local
bubble.

We have also investigated whether the observed band ratios
are fit by the emission models used. We find that with
current collisional ionization equilibrium models, depleted
abundances are necessary to be consistent with the observed
band ratios. We also show that the model predictions depend
strongly on the model version, which does little to lend
confidence to their predictions.

This work was supported by a NSF-REU site grant
(AST-0139563) to the University of Wisconsin-Madison.